Mass constraints on substellar companion candidates from the re-reducedHipparcosintermediate astrometric data: nine confirmed planets and two confirmed brown dwarfs

S. Reffert, A. Quirrenbach
2011 Astronomy and Astrophysics  
We search for the astrometric signatures of planets and brown dwarfs known from radial velocity surveys in the improved Hipparcos intermediate astrometric data provided by van Leeuwen (2007a). Our aim is to put more significant constraints on the inclination and the longitude of the ascending node than was possible before, resulting in unambiguous companion masses. We fitted the astrometric orbits of 310 substellar companions around 258 stars to the Hipparcos intermediate astrometric data. Even
more » ... rometric data. Even though the astrometric signatures of the companions cannot be detected in most cases, the Hipparcos data still provide lower limits on the inclination for all but 67 of the investigated companions, which translates into upper limits on the masses of the unseen companions. For nine companions the derived upper mass limit lies in the planetary and for 75 companions in the brown dwarf mass regime, proving the substellar nature of those objects. Two of those objects have minimum masses also in the brown dwarf regime and are thus proven to be brown dwarfs. The confirmed planets are the ones around Pollux (beta Gem b), epsilon Eri b, epsilon Ret b, mu Ara b, upsilon And c and d, 47 UMa b, HD 10647 b and HD 147513 b. The confirmed brown dwarfs are HD 137510 b and HD 168443 c. In 20 cases, the astrometric signature of the substellar companion was detected in the Hipparcos data. Of these 20 companions, three are confirmed as planets or lightweight brown dwarfs (HD 87833 b, iota Dra b, and gamma Cep b), two as brown dwarfs (HD 106252 b and HD 168443 b), and four are low-mass stars (BD -04 782 b, HD 112758 b, rho CrB b, and HD169822 b). Of the others, many are either brown dwarfs or very low mass stars. For epsilon Eri, we derive a solution which is very similar to the one obtained using Hubble Space Telescope data.
doi:10.1051/0004-6361/201015861 fatcat:coua72n7gzevhlpgcs7g3sq4vm